Notice:
Due to the conversion of some ACS WFC or HRC observations into
WFPC2,
or NICMOS observations after the loss of ACS CCD science
capability
in January, there may be an occasional discrepancy between a
proposal's
listed (and correct) instrument usage and the abstract that
follows
it.
HUBBLE
SPACE TELESCOPE - Continuing to collect World Class Science
DAILY
REPORT # 4498
PERIOD
COVERED: UT November 30 December 1, 2, 2007 (DOY 334,335,336)
OBSERVATIONS
SCHEDULED
NIC1/NIC2/NIC3
8794
NICMOS Post-SAA calibration - CR Persistence Part 5
A
new procedure proposed to alleviate the CR-persistence problem of
NICMOS.
Dark frames will be obtained immediately upon exiting the SAA
contour
23, and every time a NICMOS exposure is scheduled within 50
minutes
of coming out of the SAA. The darks will be obtained in parallel
in
all three NICMOS Cameras. The POST-SAA darks will be non- standard
reference
files available to users with a USEAFTER date/time mark. The
keyword
'USEAFTER=date/time' will also be added to the header of each
POST-SAA
DARK frame. The keyword must be populated with the time, in
addition
to the date, because HST crosses the SAA ~8 times per day so
each
POST-SAA DARK will need to have the appropriate time specified, for
users
to identify the ones they need. Both the raw and processed images
will
be archived as POST-SAA DARKs. Generally we expect that all NICMOS
science/calibration
observations started within 50 minutes of leaving an
SAA
will need such maps to remove the CR persistence from the science
images.
Each observation will need its own CRMAP, as different SAA
passages
leave different imprints on the NICMOS detectors.
WFPC2
11361
Hubble
Heritage Observations of Mars at 2007 Opposition
We
will obtain images of Mars at opposition in December 2007.
NIC3
11334
NICMOS
Cycle 16 Spectrophotometry
Observation
of the three primary WD flux standards must be repeated to
refine
the NICMOS absolute calibration and monitor for sensitivity
degradation.
So far, NICMOS grism spectrophotometry is available for
only
~16 stars with good STIS spectra at shorter wavelengths. There are
more
in the HST CALSPEC standard star data base with good STIS spectra
that
would also become precise IR standards with NICMOS absolute SED
measurements.
Monitoring the crucial three very red stars (M, L, T) for
variability
and better S/N in the IR. Apparent variability was
discovered
at shorter wavelengths during the ACS cross-calibration work
that
revealed a ~2% discrepancy of the cool star fluxes with respect to
the
hot primary WD standards. About a third of these stars are bright
enough
to do in one orbit, the rest require 2 orbits.
ACS/SBC
11323
Improved
Wavelengths Calibration of SBC Prisms
We
propose to check and improve the wavelength calibration of the SBC
PR110L
and PR130L prisms by observing an additional calibrator target
for
which observations failed in Cycle 14. Previous calibration
programs included two QSOs
at redshifts z = 0.098 (PG1404+226), z =
0.168
(PG1322+659), and z=0.234 (PB5723), but the observation of a
further
QSO at z = 0.313 (3C249.1) failed. This proposals aims to obtain
observations
of 3C249.1. The observations of PB5723 show adequate
agreement
of the wavelength of the Lyman alphaline as a function of
position
but, while the rms is around 0.5 pixel, some spectra show
evidence
of stretching of the wavelength scale. Given the steeply
increased
use of the SBC prims in Cycle 16 it is desirable to obtain
additional
observations in order to check the existing calibration,
identify
any trends with time and thus improve the SBC prism wavelength
calibration.
S/C
11320
NICMOS
Focus Monitoring Cycle 16
This
program is a version of the standard focus sweep used since cycle
7.
It has been modified to go deeper and uses more narrow filters for
improved
focus determination. A new source was added in Cycle 14 in
order
to accommodate 2-gyro mode: the open cluster NGC1850. This source
is
part of the current proposal. The old target, the open cluster
NGC3603,
will be used whenever available and the new target used to fill
the
periods when NGC3603 is not visible. Steps: a) Use refined target
field
positions as determined from cycle 7 calibrations b) Use
MULTIACCUM
sequences of sufficient dynamic range to account for defocus
c)
Do a 17-point focus sweep, +/- 8mm about the PAM mechanical zeropoint
for
each cameras 1 and 2, in 1.0mm steps. For NIC3 we step from -0.5mm
to
-9.5mm relative to mechanical zero, in steps of 1.0mm. d) Use PAM X/Y
tilt
and OTA offset slew compensations refined from previous focus
monitoring/optical
alignment activities
FGS
11212
Filling
the Period Gap for Massive Binaries
The
current census of binaries among the massive O-type stars is
seriously
incomplete for systems in the period range from years to
millennia
because the radial velocity variations are too small and the
angular
separations too close for easy detection. Here we propose to
discover
binaries in this observational gap through a Faint Guidance
Sensor
SNAP survey of relatively bright targets listed in the Galactic O
Star
Catalog. Our primary goal is to determine the binary frequency
among
those in the cluster/association, field, and runaway groups. The
results
will help us assess the role of binaries in massive star
formation
and in the processes that lead to the ejection of massive
stars
from their natal clusters. The program will also lead to the
identification
of new, close binaries that will be targets of long term
spectroscopic
and high angular resolution observations to determine
their
masses and distances. The results will also be important for the
interpretation
of the spectra of suspected and newly identified binary
and
multiple systems.
WFPC2
11202
The
Structure of Early-type Galaxies: 0.1-100 Effective Radii
The
structure, formation and evolution of early-type galaxies is still
largely
an open problem in cosmology: how does the Universe evolve from
large
linear scales dominated by dark matter to the highly non-linear
scales
of galaxies, where baryons and dark matter both play important,
interacting,
roles? To understand the complex physical processes
involved
in their formation scenario, and why they have the tight
scaling
relations that we observe today {e.g. the Fundamental Plane}, it
is
critically important not only to understand their stellar structure,
but
also their dark-matter distribution from the smallest to the largest
scales.
Over the last three years the SLACS collaboration has developed
a
toolbox to tackle these issues in a unique and encompassing way by
combining
new non-parametric strong lensing techniques, stellar
dynamics,
and most recently weak gravitational lensing, with
high-quality
Hubble Space Telescope imaging and VLT/Keck spectroscopic
data
of early-type lens systems. This allows us to break degeneracies
that
are inherent to each of these techniques separately and probe the
mass
structure of early-type galaxies from 0.1 to 100 effective radii.
The
large dynamic range to which lensing is sensitive allows us both to
probe
the clumpy substructure of these galaxies, as well as their
low-density
outer haloes. These methods have convincingly been
demonstrated,
by our team, using smaller pilot-samples of SLACS lens
systems
with HST data. In this proposal, we request observing time with
WFPC2
and NICMOS to observe 53 strong lens systems from SLACS, to obtain
complete
multi-color imaging for each system. This would bring the total
number
of SLACS lens systems to 87 with completed HST imaging and
effectively
doubles the known number of galaxy-scale strong lenses. The
deep
HST images enable us to fully exploit our new techniques, beat down
low-number
statistics, and probe the structure and evolution of
early-type
galaxies, not only with a uniform data-set an order of
magnitude
larger than what is available now, but also with a fully
coherent
and self-consistent methodological approach!
WFPC2
11178
Probing
Solar System History with Orbits, Masses, and Colors of
Transneptunian
Binaries
The
recent discovery of numerous transneptunian binaries {TNBs} opens a
window
into dynamical conditions in the protoplanetary disk where they
formed
as well as the history of subsequent events which sculpted the
outer
Solar System and emplaced them onto their present day heliocentric
orbits.
To date, at least 47 TNBs have been discovered, but only about a
dozen
have had their mutual orbits and separate colors determined,
frustrating
their use to investigate numerous important scientific
questions.
The current shortage of data especially cripples scientific
investigations
requiring statistical comparisons among the ensemble
characteristics.
We propose to obtain sufficient astrometry and
photometry
of 23 TNBs to compute their mutual orbits and system masses
and
to determine separate primary and secondary colors, roughly tripling
the
sample for which this information is known, as well as extending it
to
include systems of two near-equal size bodies. To make the most
efficient
possible use of HST, we will use a
optimally
schedule our observations.
NIC2
11142
Revealing
the Physical Nature of Infrared Luminous Galaxies at 0.3
We aim
to determine physical properties of IR luminous galaxies at
0.3<z<2.7
by requesting coordinated HST/NIC2 and MIPS 70um observations
of
a unique, 24um flux- limited sample with complete Spitzer mid-IR
spectroscopy.
The 150 sources investigated in this program have S{24um}
>
0.8mJy and their mid-IR spectra have already provided the majority
targets
with spectroscopic redshifts {0.3<z<2.7}. The proposed
150~orbits
of NIC2 and 66~hours of MIPS 70um will provide the physical
measurements
of the light distribution at the rest-frame ~8000A and
better
estimates of the bolometric luminosity. Combining these
parameters
together with the rich suite of spectral diagnostics from the
mid-IR
spectra, we will {1} measure how common mergers are among LIRGs
and
ULIRGs at 0.3<z<2.7, and establish if major mergers are the drivers
of
z>1 ULIRGs, as in the local Universe. {2} study the co-evolution of
star
formation and blackhole accretion by investigating the relations
between
the fraction of starburst/AGN measured from mid-IR spectra vs.
HST
morphologies, L{bol} and z. {3} obtain the current best estimates of
the
far- IR emission, thus L{bol} for this sample, and establish if the
relative
contribtuion of mid-to- far IR dust emission is correlated with
morphology
{resolved vs. unresolved}.
WFPC2
11130
AGNs
with Intermediate-mass Black Holes: Testing the Black Hole-Bulge
Paradigm,
Part II
The
recent progress in the study of central black holes in galactic
nuclei
has led to a general consensus that supermassive {10^6-10^9 solar
mass}
black holes are closely connected with the formation and
evolutionary
history of large galaxies, especially their bulge
component.
Two outstanding issues, however, remain unresolved. Can
central
black holes form in the absence of a bulge? And does the mass
function
of central black holes extend below 10^6 solar masses?
Intermediate-mass
black holes {<10^6 solar masses}, if they exist, may
offer
important clues to the nature of the seeds of supermassive black
holes.
Using the SDSS, our group has successfully uncovered a new
population
of AGNs with intermediate-mass black holes that reside in
low-luminosity
galaxies. However, very little is known about the
detailed
morphologies or structural parameters of the host galaxies
themselves,
including the crucial question of whether they have bulges
or
not. Surprisingly, the majority of the targets of our Cycle 14 pilot
program
have structural properties similar to dwarf elliptical galaxies.
The
statistics from this initial study, however, are really too sparse
to
reach definitive conclusions on this important new class of black
holes.
We wish to extend this study to a larger sample, by using the
Snapshot
mode to obtain WFPC2 F814W images from a parent sample of 175
AGNs
with intermediate-mass black holes selected from our final SDSS
search.
We are particularly keen to determine whether the hosts contain
bulges,
and if so, how the fundamental plane properties of the host
depend
on the mass of their central black holes. We will also
investigate
the environment of this unique class of AGNs.
WFPC2
11125
The
Dynamical Evolution of Globular Clusters
Globular
clusters evolve through dynamical interactions, with primordial
binaries
extending the time until core collapse by up to an order of
magnitude,
depending on the initial binary fraction. These dynamical
interactions
plus mass segregation causes the binary fraction to rise in
the
core but fall at larger radii. We hope to eventually test these
broad
predictions by comparing them to the binary properties for
globular
clusters at different states of evolution, defined by the ratio
of
their age to the dynamical relaxation time at the half-light radius.
The
most important unknown aspects in the modeling process are the
initial
conditions of binaries in the cluster. Here we propose to
determine
the initial binary fraction as a function of radius by
studying
three of the dynamically youngest globular clusters {NGC 5053,
NGC
5466, and NGC 5897}. The presence of binaries thickens the
Sequence
in a color-magnitude diagram, which can be detected with deep
multicolor
images.
WFPC2
11103
A
Snapshot Survey of The Most Massive Clusters of Galaxies
We
propose the continuation of our highly successful SNAPshot survey of
a
sample of 125 very X-ray luminous clusters in the redshift range
0.3-0.7.
As demonstrated by the 25 snapshots obtained so far in Cycle14
and
Cycle15 these systems frequently exhibit strong gravitational
lensing
as well as spectacular examples of violent galaxy interactions.
The
proposed observations will provide important constraints on the
cluster
mass distributions, the physical nature of galaxy-galaxy and
galaxy-gas
interactions in cluster cores, and a set of optically bright,
lensed
galaxies for further 8-10m spectroscopy. All of our primary
science
goals require only the detection and characterization of
high-surface-brightness
features and are thus achievable even at the
reduced
sensitivity of WFPC2. Because of their high redshift and thus
compact
angular scale our target clusters are less adversely affected by
the
smaller field of view of WFPC2 than more nearby systems.
Acknowledging
the broad community interest in this sample we waive our
data
rights for these observations. Due to a clerical error at STScI our
approved
Cycle15 SNAP program was barred from execution for 3 months and
only
6 observations have been performed to date - reinstating this SNAP
at
Cycle16 priority is of paramount importance to reach meaningful
statistics.
WFPC2
11079
Treasury
Imaging of Star Forming Regions in the Local Group:
Complementing
the GALEX and NOAO Surveys
We
propose to use WFPC2 to image the most interesting star-forming
regions
in the Local Group galaxies, to resolve their young stellar
populations.
We will use a set of filters including F170W, which is
critical
to detect and characterize the most massive stars, to whose hot
temperatures
colors at longer wavelengths are not sensitive. WFPC2's
field
of view ideally matches the typical size of the star-forming
regions,
and its spatial resolution allows us to measure individual
stars,
given the proximity of these galaxies. The resulting H-R diagrams
will
enable studies of star-formation properties in these regions, which
cover
largely differing metallicities {a factor of 17, compared to the
factor
of 4 explored so far} and characteristics. The results will
further
our understanding of the star-formation process, of the
interplay
between massive stars and environment, the properties of dust,
and
will provide the key to interpret integrated measurements of
star-formation
indicators {UV, IR, Halpha} available for several
hundreds
more distant galaxies. Our recent deep surveys of these
galaxies
with GALEX {FUV, NUV} and ground-based imaging {UBVRI, Halpha,
[OIII]
and [SII]} provided the identification of the most relevant SF
sites.
In addition to our scientific analysis, we will provide catalogs
of
HST photometry in 6 bands, matched corollary ground-based data, and
UV,
Halpha and IR integrated measurements of the associations, for
comparison
of integrated star-formation indices to the resolved
populations.
We envisage an EPO component.
WFPC2
11029
WFPC2
CYCLE 15 Intflat Linearity Check and Filter Rotation Anomaly
Monitor
Intflat
observations will be taken to provide a linearity check: the
linearity
test consists of a series of intflats in F555W, in each gain
and
each shutter. A combination of intflats, visflats, and earthflats
will
be used to check the repeatability of filter wheel motions.
{Intflat
sequences tied to decons, visits 1-18 in prop 10363, have been
moved
to the cycle 15 decon proposal xxxx for easier scheduling.} Note:
long-exposure
WFPC2 intflats must be scheduled during ACS anneals to
prevent
stray light from the WFPC2 lamps from contaminating long ACS
external
exposures.
WFPC2
11027
Visible
Earth Flats
This
proposal monitors flatfield stability. This proposal obtains
sequences
of Earth streak flats to construct high quality flat fields
for
the WFPC2 filter set. These flat fields will allow mapping of the
OTA
illumination pattern and will be used in conjunction with previous
internal
and external flats to generate new pipeline superflats. These
Earth
flats will complement the Earth flat data obtained during cycles
4-14.
WFPC2
11020
Cycle
15 Focus Monitor
The
focus of HST is measured primarily with ACS/HRC over full CVZ orbits
to
obtain accurate mean focus values via a well sampled breathing curve.
Coma
and astigmatism are also determined from the same data in order to
further
understand orbital effects on image quality and optical
alignments.
To monitor the stability of ACS to WFPC2 relative focii,
we've
carried over from previous focus monitor programs parallel
observations
taken with the two cameras at suitable orientations of
previously
observed targets, and interspersed them with the HRC CVZ
visits.
WFPC2
11011
Dissecting
An Accretion Disk
We
will use 5 epochs of CXO and HST imaging to determine the X-ray and
UV size
of the accretion disk of the lensed quasar RXJ1131--1231 using
microlensing.
Based on preliminary data, we find that the X-ray source
is
roughly 1/10 the size of the accretion disk in the rest-frame B-band.
The
new observations will significantly reduce the uncertainties in this
estimate,
provide a comparison between the size of the X-ray source and
the
size of the accretion disk in the rest frame ultraviolet, and have
the
signal-to-noise ratio necessary to begin examining the size of the
hard
and soft-band X-ray emission regions separately. The results will
quantitatively
test accretion disk theory and X-ray emission mechanisms.
WFPC2
10915
ACS
Nearby Galaxy Survey
Existing
HST observations of nearby galaxies comprise a sparse and
highly
non-uniform archive, making comprehensive comparative studies
among
galaxies essentially impossible. We propose to secure HST's
lasting
impact on the study of nearby galaxies by undertaking a
systematic,
complete, and carefully crafted imaging survey of ALL
galaxies
in the Local Universe outside the Local Group. The resulting
images
will allow unprecedented measurements of: {1} the star formation
history
{SFH} of a >100 Mpc^3 volume of the Universe with a time
resolution
of Delta[log{t}]=0.25; {2} correlations between spatially
resolved
SFHs and environment; {3} the structure and properties of thick
disks
and stellar halos; and {4} the color distributions, sizes, and
specific
frequencies of globular and disk clusters as a function of
galaxy
mass and environment. To reach these goals, we will use a
combination
of wide-field tiling and pointed deep imaging to obtain
uniform
data on all 72 galaxies within a volume-limited sample extending
to
~3.5 Mpc, with an extension to the M81 group. For each galaxy, the
wide-field
imaging will cover out to ~1.5 times the optical radius and
will
reach photometric depths of at least 2 magnitudes below the tip of
the
red giant branch throughout the limits of the survey volume. One
additional
deep pointing per galaxy will reach SNR~10 for red clump
stars,
sufficient to recover the ancient SFH from the color-magnitude
diagram.
This proposal will produce photometric information for ~100
million
stars {comparable to the number in the SDSS survey} and uniform
multi-
color images of half a square degree of sky. The resulting
archive
will establish the fundamental optical database for nearby
galaxies,
in preparation for the shift of high- resolution imaging to
the
near-infrared.
ACS/SBC
10907
New
Sightlines for the Study of Intergalactic Helium: A Dozen
High-Confidence,
UV-Bright Quasars from SDSS/GALEX
The
reionization of intergalactic helium is thought to have occurred
between
redshifts of about 3 and 4. Detailed study of HeII Lyman-alpha
absorption
toward a handful quasars at 2.7<z<3.3 demonstrates the great
potential
of such probes of the IGM, but the current critically-small
sample
limits confidence in resulting cosmological inferences. The
requisite
unobscured quasar sightlines to high-redshift are extremely
rare,
especially due to severe absorption in random intervening
Lyman-limit
systems, but SDSS provides thousands of z>3.1 quasars
potentially
suitable for HeII studies. We have cross-correlated SDSS
quasars
with GALEX UV sources to obtain a dozen new, very
high-confidence,
candidate quasars/sightlines {z=3.1 to 4.1} potentially
useful
for detailed HeII studies even with current HST instruments. We
propose
brief, 2-orbit per target, reconnaissance spectral exposures
with
the ACS SBC prism to definitively verify UV flux down to the HeII
break.
Our combined SDSS/GALEX selection insures a very high-yield of
confirmations,
as the quasars are already known to be UV-bright from
broadband
GALEX images. The additional sightlines, extending to very
high-redshift,
will directly enable ensemble spectral stacks, as well as
long
exposure follow-up spectra, at high S/N with the ACS/SBC
ultraviolet
prisms {or perhaps STIS or
measure
the spectrum and evolution of the ionizing background radiation,
the
evolution of HeII opacity, and the density of intergalactic baryons.
NIC2
10896
An
Efficient ACS Coronagraphic Survey for Debris Disks around Nearby
Stars
We
propose to finish our Cycle 11 optical survey for nearby debris disks
using
the ACS/HRC coronagraph. Out of 43 orbits originally proposed for
the
survey, 23 orbits were allocated, leading to a survey of 22 stars,
from
which two new debris disks were imaged for the first time. Our
analysis
of the initial survey gives an empirical estimate for the
detection
rate of debris disks relative to heliocentric distance and
dust
optical depth. Our target list for Cycle 15 is now optimized to
yield
more frequent disk detections. Likewise our observing strategy is
improved
to maximize sensitivity per telescope orbit allocated.
Therefore
we present the most efficient survey possible. The scientific
motivation
is to obtain scattered light images of previously unresolved
debris
disks to determine their viewing geometry and physical
architecture,
both of which may characterize the underlying planetary
system.
We choose 25 debris disk targets for which we predict a
detection
rate of 25% ? 5%. Four targets have extrasolar planets from
which
the viewing geometry revealed by a disk detection will resolve the
v
sin{i} ambiguity in the planet masses. These targets present the
remarkable
opportunity of finally seeing a debris disk in system with
known
planets.
FLIGHT
OPERATIONS SUMMARY:
Significant
Spacecraft Anomalies: (The following are preliminary reports
of
potential non-nominal performance that will be investigated.)
HSTARS:
11082
- REAcq (1,2,2) failed to RGA Hold
At AOS (334/23:25:15) observed that REAcq (1,2,2) scheduled
from
22:59:42 - 23:07:17 had failed to RGA Hold due to QSTOP &
QF1STOPF flags
on FGS 1. No 486 ESB messages were received. Due to LOS, the data
from
OBAD 1 & 2 is unavailable till an engineering data dump is
performed.
OBAD MAP data showed the following results: V1 -13.66, V2 -5.48,
V3
-5.82, RSS 15.83.
11084
- REACQ(1,2,1) failed, Search Radius Limit exceeded on FGS 1
REACQ(1,2,1) at 335/21:25:44 failed at 21:31:03 with search radius
limit
exceeded on FGS 1. Three 486 status buffer 1805
(T2G_MOVING_TARGET_DETECTED) and one "A05" message (FGS
Coarse Track
failed- search Radius Limit exceeded) were received. Primary
GSACQ(1,2,1) at 19:51:59 was successful.
COMPLETED
OPS REQUEST: (None)
COMPLETED
OPS NOTES: (None)
SCHEDULED
SUCCESSFUL
FGS
GSacq
24
24
FGS
REacq
14
12
OBAD
with Maneuver
76
76
SIGNIFICANT
EVENTS: (None)